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Many multiple-planet systems have been found by the Kepler transit survey andvarious radial velocity (RV) surveys. Kepler planets show an asymmetricfeature, namely, there are small but significant deficits/excesses of planetpairs with orbital period spacing slightly narrow/wide of the exact resonance,particularly near the first order mean motion resonance (MMR), such as 2:1 and3:2 MMR. Similarly, if not exactly the same, an asymmetric feature (pileup wideof 2:1 MMR) is also seen in RV planets, but only for massive ones. Weanalytically and numerically study planets' orbital evolutions near and in theMMR. We find that their orbital period ratios could be asymmetricallydistributed around the MMR center regardless of dissipation. In the case of nodissipation, Kepler planets' asymmetric orbital distribution could be partlyreproduced for 3:2 MMR but not for 2:1 MMR, implying that dissipation might bemore important to the latter. The pileup of massive RV planets just wide of 2:1MMR is found to be consistent with the scenario that planets formed separatelythen migrated toward the MMR. The location of the pileup infers a K value of1-100 on the order of magnitude for massive planets, where K is the dampingrate ratio between orbital eccentricity and semimajor axis during planetmigration.

Asymmetric Orbital Distribution near Mean Motion Resonance: Application to Planets Observed by Kepler and Radial Velocities